Journal ArticleThe Distance to the S147 Supernova RemnantKochanek, C S; Raymond, John C; Caldwell, Nelson<title>Abstract</title> <p>In the absence of a parallax distance to a pulsar or a surviving binary in a supernova remnant (SNR), distances to Galactic SNRs are generally very uncertain. However, by combining Gaia data with wide-field, multifiber echelle spectroscopy, it is now possible to obtain accurate distances to many SNRs with limited extinction by searching for the appearance of high-velocity Ca<sc>ii</sc>or Na<sc>i</sc>absorption lines in hot stars as a function of distance. We demonstrate this for the SNR S147 using the spectra of 259 luminous blue stars. We obtain a median distance of 1.37 kpc (1.30–1.47 kpc at 90% confidence), which is consistent with the median parallax distance to the pulsar of 1.46 kpc (1.12–2.10 kpc at 90% confidence) but with significantly smaller uncertainties. Our distance is also consistent with the distance to the candidate unbound binary companion in this SNR, HD 37424 at a photogeometric distance of 1.45 kpc (1.40–1.50 kpc at 1<italic>σ</italic>). The presence of high-velocity absorption lines is correlated with the H<italic>α</italic>/O [<sc>iii</sc>] emission-line flux of the SNR but not with the radio flux.</p>The Astrophysical Journal2024-06-0110526444The Astrophysical Journal9682940004-637Xhttps://doi.org/10.3847/1538-4357/ad44932307385National Science Foundation